Search arXiv⌕ Search

arXiv · 2610.39473

Cosmological axion-photon interactions with a nonminimal dark gauge sector

Abstract

We study the cosmological evolution of radiation and dark radiation with nonminimal axion-photon-dark photon couplings. The Chern-Simons-type axion-gauge field interactions between the dark and visible sectors can induce energy conversion between photons and dark photons as well as polarization rotation during the propagation of radiation, leading to CMB spectral distortions and cosmic birefringence. Using the observed CMB monopole spectrum, we constrain the photon-dark photon energy conversion fraction, which is determined by the coupling constants and the evolution of the axion field. We further show that the parity-odd mixing interaction $ϕF\tilde{B}$ can partially relax the constraints on the standard axion-photon coupling, $ϕF\tilde{F}$, derived from the current observational limits of the cosmic birefringence angle.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Hao Jiao, Dong-Won Jung, Nils A. Nilsson. 2026-10-29. Cosmological axion-photon interactions with a nonminimal dark gauge sector. https://arxiv.org/abs/2610.39473

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Analytic Gravitational Wave Spectrum in Next-to-Minimal Bouncing Cosmology

Bouncing cosmology offers a singularity-free alternative to inflation. However, its minimal realization, known as minimal bouncing cosmology (MBC), comprises only four cosmic phases and produces a stochastic gravitational-wave background (SGWB) with a single power-law spectrum. Interpreting the pulsar timing array (PTA) signal within this framework faces tension with the $ΔN_{\rm eff}$ bound and has required trans-Planckian bounce energies, restricting its observational viability. In this work, we propose next-to-minimal bouncing cosmology (NMBC) by adding an earlier phase of cosmic evolution to MBC. Using our previously developed primordial gravitational-wave propagation-matrix method, with an improved matching prescription, we derive explicit analytic expressions for the resulting SGWB spectrum. The spectrum takes a broken power-law form: the low- and high-frequency tilts are determined by the equations of state of the additional and original contraction phases, respectively, while the spectral amplitudes depend jointly on these equations of state and the characteristic transition-time scales. This additional freedom allows a PTA-band signal to coexist with a scale-invariant or red-tilted high-frequency branch, providing a way to satisfy the $ΔN_{\rm eff}$ bound. For the scale-invariant high-frequency branch, a pointwise benchmark using the adopted $ΔN_{\rm eff}$ radiation budget gives $ρ_{s\downarrow}^{1/4}\lesssim2.65\,m_{\rm pl}$, where $m_{\rm pl}$ is the reduced Planck mass. This provides a conservative comparison estimate for the setup considered here, since integrating the spectrum over the adopted illustrative frequency interval gives a tighter bound. The resulting upper limit is therefore of order the reduced Planck scale. please refer to the PDF for the full abstract.

astro-ph.CO↗

photo-3x2-pt: Cosmology from cosmic shear and galaxy clustering with a single photometric galaxy catalog

We perform a joint cosmological analysis using angular power spectra of galaxy clustering, galaxy-shear cross correlation, and cosmic shear (hereafter referred to as photo-3x2-pt) measured from the Hyper Suprime-Cam year-3 (HSC-Y3) weak lensing shape catalog. We employ the pseudo-$C_\ell$ method to measure these power spectra and use the template deprojection method to mitigate systematics in the galaxy density maps. We perform a standard Bayesian likelihood analysis for cosmological inference based on the measured photo-3x2-pt, including contributions from intrinsic alignments of galaxies, galaxy clustering bias, lensing magnification effect, baryonic feedback effect, and source redshift distribution errors. For a flat cold dark matter model, we find a 68% credible interval of $0.76 \le S_8 \le 0.81$. This result is consistent with the HSC-Y3 cosmic shear analyses (Dalal et al. 2023, Li et al. 2023) but is $\sim 25$% tighter. We also find that the measured B-mode power spectra are consistent with zero. We also perform a performance test using mock catalogs that mimic the HSC-Y3 data to validate our photo-3x2-pt analysis. Through Bayesian parameter inference of mock data, we verify that unbiased estimates can be obtained for the key cosmological and nuisance parameters, including $S_8$, intrinsic alignment model parameters, galaxy clustering bias, and shift parameters of the source redshift distributions.

astro-ph.CO↗

Conformally Coupled Scalar- Field Dark Energy: Cosmological Dynamics with Early- and Late- Measurements

In this work, the cosmology of the conformal interacting dark energy model is investigated by introducing a scalar field representing dark energy (DE) coupled to dark matter (DM) via a conformal transformation. This coupling yields a class of scalar+tensor theories; the interaction term ${Q}$, which indicates the flow of energy between the dark sectors, is proportional to the trace of the energy-momentum tensor of the DM fluid, $T^{\mathrm{DM}}_{μν}$, as ${Q}=\frac{C'(ϕ)}{2C(ϕ)}g^{μν}T^{\mathrm{DM}}_{μν}$, where $C(ϕ)$ is the conformal function of a scalar potential (coupling) field. We assume the power-law parametrization $C(ϕ)\propto (1+ϕ)^m$, with $m$ as the coupling parameter, and determine the direction and magnitude of energy flow between the DM and DE scalar-field components. We model DE in three scenarios: conformally interacting dark energy (CIDE) coupled to a scalar field, uncoupled scalar+field DE (UCSFDE), and standard $ Λ$CDM models. We confront these models with cosmological measurements to test the viability of CIDE and UCSFED against $Λ$CDM and constrain them using a combination of early and late time data, namely: Cosmic Microwave Background measurements from Planck 2018 Legacy (\texttt{CMB}); Baryon Acoustic Oscillation (BAO) data from the Dark Energy Survey (\texttt{ DESI DR2 DR2 BAO}); and Supernova Type Ia distance compilations (\texttt{PantheonPlus, PantheonPlus + SH0ES, Union3}, and \texttt{DES+Dovekie}). We perform parameter inference with Monte Carlo Markov Chain (\texttt{MCMC}) simulations using \texttt{COBAYA} and a modified \texttt{CLASS} ...

astro-ph.CO↗